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The nuclear and extended mid-infrared emission of Seyfert Galaxies I. García-Bernete, C. Ramos Almeida, J. A. Acosta-Pulido, et al., 2016, MNRAS, submitted AGN: what's in a name?, Garching, 2016 The central engines of Active Galactic Nuclei (AGN) Unified Model (Antonucci 1993) The AGN type depends on orientation Seyfert torus size ~ few pc (Burtscher et al. 2013; García-Burillo et al. 2016) The torus absorbs the intrinsic AGN radiation and re-emits it in the IR, peaking in the MIR Orientation Credit: W. Steffen (UNAM) The central engines of Active Galactic Nuclei (AGN) Unified Model (Antonucci 1993) The AGN type depends on orientation Seyfert torus size ~ few pc (Burtscher et al. 2013; García-Burillo et al. 2016) The torus absorbs the intrinsic AGN radiation and re-emits it in the IR, peaking in the MIR Orientation Credit: W. Steffen (UNAM) The central engines of Active Galactic Nuclei (AGN) Unified Model (Antonucci 1993) The AGN type depends on orientation Seyfert torus size ~ few pc (Burtscher et al. 2013; García-Burillo et al. 2016) The torus absorbs the intrinsic AGN radiation and re-emits it in the IR, peaking in the MIR Orientation Credit: W. Steffen (UNAM) The central engines of Active Galactic Nuclei (AGN) Unified Model (Antonucci 1993) The AGN type depends on orientation Seyfert torus size ~ few pc (Burtscher et al. 2013; García-Burillo et al. 2016) The torus absorbs the intrinsic AGN radiation and re-emits it in the IR, peaking in the MIR Orientation Black Hole Accretion disk Clumpy torus MIR Cold dust FIR Credit: W. Steffen (UNAM) Mid-IR imaging: space (Spitzer/IRAC) vs. ground (Gemini/T-ReCS) observations Díaz-Santos (2009, PhD) Mid-IR imaging: space (Spitzer/IRAC) vs. ground (Gemini/T-ReCS) observations Díaz-Santos (2009, PhD) IRAC 8 micron Sample selection 9 Month Swift/BAT AGN catalog Very hard 14-195 keV band One of the most complete to date IRAC 8 micron Sample selection 9 Month Swift/BAT AGN catalog Very hard 14-195 keV band One of the most complete to date Seyferts and distance limit Gemini/MICHELLE 8-10 m-class ground-based telescopes N-band: resolution ~0.3'' DL<40 Mpc → resolution< 50 pc IRAC 8 micron Sample selection 9 Month Swift/BAT AGN catalog Very hard 14-195 keV band One of the most complete to date Seyferts and distance limit Gemini/MICHELLE 8-10 m-class ground-based telescopes N-band: resolution ~0.3'' DL<40 Mpc → resolution< 50 pc 24 Seyfert galaxies Statistically significant results Nuclear and circumnuclear MIR emission Nuclear & circumnuclear fluxes Compactness factor Nuclear fluxes (inner ~70 pc)→ PSF subtraction (nuclear/total flux ratio) Nuclear fluxes at 8 micron The sample is dominated by circumnuclear MIR emission with low surface brightness The extended emission is ~30% of the total emission Circumnuclear emission = total – nuclear emission ~25% Sy 1 and ~30% Sy 2 It is important to perform visual classification to take into account this emission Parsec-scale morphologies MIR morphologies classification (visual & quantitative) Comparison subarcsecond vs MIR morphologies on scales of ~400 pc Visual classification (by eye) Quantitative classification: Compactness factor and PSF-sub residuals 75-79% of the sample show extended morphologies arcsecond res. data Only few galaxies have similar structures For the majority of the galaxies, the IRAC PSF is larger than the HR extended emission The HR data is important to characterize the circumnuclear MIR emission Parsec-scale morphologies Are the MIR morphologies related to galaxy inclination and/or luminosity? Point-like MIR morphologies found in face-on or moderately-inclined galaxies Extended MIR morphologies found in galaxies at different inclinations We do not find a dependence of the MIR morphologies on X-ray luminosity Kpc-scale morphologies Arcsecond res. data Kpc-scale morphologies Arcsecond res. data Galaxies with high S/N extended emission Similar structures and orientations Origin of the heating source of the MIR extended emission vs subarcsecond res. data Spitzer/IRS spectra Kpc-scale morphologies Arcsecond vs subarcsecond res. data Galaxies with high S/N extended emission Similar structures and orientations Origin of the heating source of the MIR extended emission N-band Q-band Spitzer/IRS spectra AGN-dominated systems have more compact MIR emission (300±100 pc) than SF dominated systems (600±700 pc) Kpc-scale morphologies Arcsecond vs subarcsecond res. data Galaxies with high S/N extended emission Similar structures and orientations Origin of the heating source of the MIR extended emission Spitzer/IRS spectra AGN-dominated systems have more compact MIR emission (300±100 pc) than SF dominated systems (600±700 pc) Comparison with normal galaxies Using IRAC data 70 nearby normal galaxies (SINGs sample) The total MIR luminosity of Seyfert galaxies is higher than in normal galaxies N-band Q-band Subtracting the nuclear emission → remains larger than normal galaxies Extra-contribution of AGN-heated dust MIR correlations with AGN and SF indicators Circumnuclear emission 14-195 keV 2-10 keV Nuclear emission Nuclear and circumnuclear MIR emission: tight correlation with X-rays → AGN activity Sy 1 and Sy 2 are consistent with each other → 8 micron nuclear fluxes are nearly isotropic MIR correlations with AGN and SF indicators Circumnuclear emission [Ne II]SF [O IV] Nuclear emission Tight correlation with X-rays and [O IV], and weak correlation with [Ne II]SF → nuclear and circumnuclear MIR emission are AGN-dominated Conclusions ● The majority of the galaxies (75-59%) show extended morphologies ● This extended emission has low surface brightness → (~30% of the total) ● AGN-dominated systems have more compact extended MIR emission than SF-dominated systems ● Tight correlations with X-rays and [O IV], and weak correlation with [Ne II]SF → 8 micron nuclear fluxes (~70 pc) in our sample are AGN-dominated ● Practically the same correlations with larger scatter for the circumnuclear emission → AGN dominates the MIR emission in the inner ~ 400 pc (with some contribution of SF) I. García-Bernete, C. Ramos Almeida, J. A. Acosta-Pulido, et al., 2016, MNRAS, submitted Email: [email protected] Next... Study of the torus properties of this complete sample of Seyfert galaxies Nuclear IR fluxes and high angular resolution MIR spectra NGC 2992 Are the covering factors of Sy1 and Sy2 ≠ ? García-Bernete et al. (2015) Ramos Almeida et al. (2014) Email: [email protected] Nuclear MIR emission Nuclear fluxes Nuclear fluxes (inner ~70 pc)→ PSF subtraction Nuclear fluxes at 8 micron 1) Match the PSF star to the galaxy peak 100 % (oversubtracted) 2) Subtract different percentages of the galaxy peak emission 3) Find non-oversubtracted residuals 1-D profile Subtraction residuals Nuclear MIR emission Nuclear fluxes Nuclear fluxes (inner ~70 pc)→ PSF subtraction (HR observations with ≠ filters) Spitzer/IRS spectral decomposition Spitzer/IRS spectrum Nuclear fluxes as priors Model AGN PAH Homogeneous nuclear fluxes at 8 micron
